Detection of a large amount of diffuse extraplanar dust in NGC 891

Seon, Kwang‐Il; Witt, A. N.

doi:10.1017/s1743921312008915

Cited by 1 publication

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“…More recently, Seon & Witt (2012) have reported on the discovery of a UV halo due to the diffuse dust present above the galactic plane of NGC 891 and Seon et al (2014), using a 3D radiative transfer model, have found that the UV halo is well reproduced by a model with two exponential dust discs, one with a scaleheight of 0.2-0.25 kpc and a wider component with a scaleheight of 1.2-2.0 kpc.…”

Section: Introductionmentioning

confidence: 99%

Halo dust detection around NGC 891

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Bianchi

Hunt

et al. 2016

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Context. Observations of edge-on galaxies allow us to investigate the vertical extent and properties of dust, gas and stellar distributions. NGC 891 has been studied for decades and represents one of the best studied cases of an edge-on galaxy. Aims. We use deep Photoconductor Array Camera and Spectrometer (PACS) data together with Infrared Array Camera (IRAC), Multiband Imaging Photometer for Spitzer (MIPS) and Spectral and Photometric Imaging Receiver (SPIRE) data to study the vertical extent of dust emission around NGC 891. We also test for the presence of a more extended, thick dust component. Methods. By performing a convolution of an intrinsic vertical profile emission with each instrument point spread function (PSF) and comparing it with observations we derived the scale height of a thin and thick dust-disc component.Results. The emission is best fit with the sum of a thin and a thick dust component for all wavelengths considered. The scale height of both dust components shows a gradient goes from 70 μm to 250 μm. This could be due either to a drop in dust heating (and thus the dust's temperature) with the distance from the plane, or to a sizable contribution (∼15-80%) of an unresolved thin disc of hotter dust to the observed surface brightness at shorter wavelengths. The scale height of the thick dust component, using observations from 70 μm to 250 μm, has been estimated at (1.44 ± 0.12) kpc, which is consistent with previous estimates (i.e. extinction and scattering in optical bands and mid-infrared (MIR) emission). The amount of dust mass at distances greater than ∼2 kpc from the midplane represents 2-3.3% of the total galactic dust mass, and the abundance of small grains relative to large grains is almost halved compared to levels in the midplane. Conclusions. The paucity of small grains high above the midplane might indicate that dust is hit by interstellar shocks or galactic fountains and entrained together with gas. The halo dust component is likely to be embedded in an atomic/molecular gas and heated by a thick stellar disc.

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Section: Introductionmentioning

confidence: 99%